Although simulations have predicted the presence of the CGM around high-\(z\)  galaxies, most of the observational \(\mbox{Ly$\alpha $}\)  halo studies so far have focused on LAEs [1]}, [2]}. Only \(\simeq \)  10 to 30% of star-forming galaxies are LAEs at \(z\simeq 3\) –6 [3]}. \(\mbox{Ly$\alpha $}\)  haloes around UV-selected galaxies (Lyman break galaxies, LBGs) have previously been studied with NB stacks, which are biased s overdense regions [4]}, [5]}, and stacking analyses cannot provide information on the individual presence of \(\mbox{Ly$\alpha $}\)  haloes. The sample in KBSS-KCWI (Keck Baryonic Structure Survey using the KCWI) includes continuum-selected galaxies as well as LAEs, and their sample construction is not easy to characterize [6]}. Therefore, it is still unknown whether star-forming galaxies such as UV-selected galaxies generally have a \(\mbox{Ly$\alpha $}\)  halo. To minimize biases s LAEs and LBGs in overdense regions, a spectroscopically complete sample without preselection on the \(\mbox{Ly$\alpha $}\)  emission basis is required. Moreover, only the large field of view of MUSE with a long integration time enables us to do a volume-limited search for diffuse CGM emission at high redshifts.
